Latitudinal distribution of solar wind velocity and its relation to solar EUV corona
Abstract
The solar wind velocity in high heliographic latitudes up to 64°N is derived from the interplanetary scintillation of 3C48 in 1972 and 1973, and the relation between latitudinal distribution of the solar wind velocity and of the brightness of solar EUV corona is examined. In May-June 1972 the solar wind velocity tended to increase with increasing heliographic latitude of the source of observed solar wind, while the intensity of the EUV corona weakened with increasing latitude. In May-June 1973 the solar wind velocity did not noticeably increase with latitude, and average brightness of the EUV corona in low and high latitudes was approximately the same. Hence it is suggested that the latitudinal distribution of the solar wind velocity is inversely related to the brightness distribution of the solar EUV corona.
- Publication:
-
Journal of Geophysical Research
- Pub Date:
- 1974
- DOI:
- 10.1029/JA079i025p03841
- Bibcode:
- 1974JGR....79.3841W
- Keywords:
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- Particles and Fields-Interplanetary Space: Solar wind plasma;
- Solar Physics;
- Astrophysics;
- and Astronomy: Corona